Figure 3.
![Post-engulfment [Fe/H] abundances over time for a 1 M⊙mesa model that underwent accretion of a 1 M⊕ planet under different conditions: the standard post-ZAMS near-instantaneous engulfment scenario (gray–dashed), an LHB-like scenario (blue), and a disc accretion-like scenario (navy). The abundances of comparison mesa models with no accretion were subtracted off.](https://oup.silverchair-cdn.com/oup/backfile/Content_public/Journal/mnras/518/4/10.1093_mnras_stac3435/1/stac3435fig3.jpeg?Expires=1749834511&Signature=xopthwD1hcHu-EKqM4C5YDtXzdvjjXDJXcwQ4q3vk1jn145DGOwncoL08h0wqmFf5HLtweQm5slkQYu5l3ty~nhbSk2lbOlbpwbrfwrHlSnSX~ejhyNs67bbxwdhMk5EatzYVMLdXgkbYnOVBLcPjHEDZEOqMv52hZQAV6GGqR88x~FwNw2RfBg39ZG3Ol6f4gmIIwebzLVmhRk7GcWd6LJHL-ylHnttatJnC87KzHFWtdvi29yC2ZdNp1fHMNpzsHy5zMncnSxinVWJ3AKyUuRiTn4b1PuPx3DX3qXfLMbwOBlN58Pzrsnu8SFHJaTR3Tim5hT977j060LGLQfvXg__&Key-Pair-Id=APKAIE5G5CRDK6RD3PGA)
Post-engulfment [Fe/H] abundances over time for a 1 M⊙mesa model that underwent accretion of a 1 M⊕ planet under different conditions: the standard post-ZAMS near-instantaneous engulfment scenario (gray–dashed), an LHB-like scenario (blue), and a disc accretion-like scenario (navy). The abundances of comparison mesa models with no accretion were subtracted off.
